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High-energy neutrino emission in gravitational collapses
High Energy Astrophysical Phenomena · Submitted 2 Oct 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We approximately obtain the number of GeV antineutrino events (\gtrsim 1) in an ordinary detector such as Kamiokande and total energy of neutrino flux (\gtrsim 10^{53} erg), as a function of collapsing star mass.
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The abstract, sentence by sentence
In this article, we present a study of high-energy neutrino emission in gravitational collapse. A compact star is treated as a complete degenerate Fermi gas of neutrons, protons and electrons. In gravitational collapse, its density reaches the thresholds for muon and pion productions, leading to high-energy neutrinos production. By using adiabatic approximation that macroscopic collapsing processes are much slower than microscopic processes of particle interactions, we adopt equilibrium equations of microscopic processes to obtain the number of neutrino productions. Assuming 10% of variation in gravitational binding energy converted to the energy of produced neutrinos, we obtain fluxes of 10MeV electron-neutrinos and GeV electron and muon neutrinos. In addition, we compute the ratio (< 1) of total muon neutrino number to the total electron neutrino number at the source and at the Earth considering neutrino oscillations. We approximately obtain the number of GeV antineutrino events (\gtrsim 1) in an ordinary detector such as Kamiokande and total energy of neutrino flux (\gtrsim 10^{53} erg), as a function of collapsing star mass.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In this article, we present a study of high-energy neutrino emission in gravitational collapse. | contribution 0.99 | 0.86 | 0.04 | asserted 0.66 |
| s1 | A compact star is treated as a complete degenerate Fermi gas of neutrons, protons and electrons. | method 0.96 | 0.29 | 0.02 | asserted 1.00 |
| s2 | In gravitational collapse, its density reaches the thresholds for muon and pion productions, leading to high-energy neutrinos production. | background 0.56 | 0.33 | 0.23 | asserted 1.00 |
| s3 | By using adiabatic approximation that macroscopic collapsing processes are much slower than microscopic processes of particle interactions, we adopt equilibrium equations of microscopic processes to obtain the number of neutrino productions. | method 1.00 | 0.88 | 0.04 | asserted 0.99 |
| s4 | Assuming 10% of variation in gravitational binding energy converted to the energy of produced neutrinos, we obtain fluxes of 10MeV electron-neutrinos and GeV electron and muon neutrinos. | result 0.96 | 0.94 | 0.30 | asserted 1.00 |
| s5 | In addition, we compute the ratio (< 1) of total muon neutrino number to the total electron neutrino number at the source and at the Earth considering neutrino oscillations. | result 0.86 | 0.94 | 0.12 | asserted 0.99 |
| s6 | We approximately obtain the number of GeV antineutrino events (\gtrsim 1) in an ordinary detector such as Kamiokande and total energy of neutrino flux (\gtrsim 10^{53} erg), as a function of collapsing star mass. | result 0.99 | 0.94 | 0.28 | asserted 0.94 |
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Original abstract
In this article, we present a study of high-energy neutrino emission in gravitational collapse. A compact star is treated as a complete degenerate Fermi gas of neutrons, protons and electrons. In gravitational collapse, its density reaches the thresholds for muon and pion productions, leading to high-energy neutrinos production. By using adiabatic approximation that macroscopic collapsing processes are much slower than microscopic processes of particle interactions, we adopt equilibrium equations of microscopic processes to obtain the number of neutrino productions. Assuming 10% of variation in gravitational binding energy converted to the energy of produced neutrinos, we obtain fluxes of 10MeV electron-neutrinos and GeV electron and muon neutrinos. In addition, we compute the ratio (< 1) of total muon neutrino number to the total electron neutrino number at the source and at the Earth considering neutrino oscillations. We approximately obtain the number of GeV antineutrino events (\gtrsim 1) in an ordinary detector such as Kamiokande and total energy of neutrino flux (\gtrsim 10^{53} erg), as a function of collapsing star mass.
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What it cites · 19 sentences without a confident label
Uses data or values from 1 paper
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The cross section of GeV antineutrinos interaction with a proton approximately is $σ≈10^-37cm^2$ [ref] .
Neutrino masses and mixings and... · Detection of neutrinos · 1.00
Cites as background 1 paper
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Kilometer-scale neutrino detectors such as IceCube are constructed to observe these high-energy neutrinos [ref] .
Astroparticle Physics with High Energy Neutrinos: from AMANDA to IceCube · introduction · 0.85
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